具有爆发日珥、C-耀斑和EUV变暗的快边CME的分析和解释
Analysis and interpretation of a fast limb CME with eruptive prominence, C-flare and EUV dimming
摘要：
日冕物质抛射或CME是大型的动力学日冕事件。一个快临日冕物质抛射的质量平衡和运动学，包括它的日珥祖先和相关的耀斑，将与计算的磁结构进行比较，以寻找它们的起源和影响。利用多波长地基和星载观测资料，结合盘上和盘外观测资料，对2003年12月2日发生的一次快速W型临边日冕物质抛射事件进行了研究。它的爆发日珥是用南峰全H-α线通量成像日冕仪在高节奏下测量的。对来自空间仪器的EUV图像进行了处理，包括差分成像。利用SOHO/LASCO影像研究了质量过剩和运动。一个快速明亮的扩展日冕环被确定在该地区稍后记录的GOES作为C7.2耀斑，随后的增亮和加速阶段的喷发物质的冷和热的组件。在极紫外通道中，总的日冕辐射通量下降了5%，揭示了在边缘和上方的巨大变暗效应。1小时后观察到的典型的三部分结构显示了一个形状类似于爆发的灯丝/日珥的核心。逃逸CME的总测量质量（来自C2 LASCO观测的1.5x10 - 16 g）肯定超过逃逸冷日珥物质的估计质量，尽管分析Ha爆发日珥的假设，以及几天前观察到的相应的极紫外暗丝，使这一评估不确定的因素2。从目前的自由外推，我们讨论了磁中性表面的形状和一个可能的情况下导致的不稳定性，包括小尺度动力学内部和周围的灯丝。
英文摘要：
Coronal Mass ejections or CMEs are large dynamical solar-corona events. The mass balance and kinematics of a fast limb CME, including its prominence progenitor and the associated flare, will be compared with computed magnetic structures to look for their origin and effect. Multi-wavelength ground-based and space-borne observations are used to study a fast W-limb CME event of December 2, 2003, taking into account both on and off disk observations. Its erupting prominence is measured at high cadence with the Pic du Midi full H-alpha line-flux imaging coronagraph. EUV images from space instruments are processed including difference imaging. SOHO/LASCO images are used to study the mass excess and motions. A fast bright expanding coronal loop is identified in the region recorded slightly later by GOES as a C7.2 flare, followed by a brightening and an acceleration phase of the erupting material with both cool and hot components. The total coronal radiative flux dropped by 5 percent in the EUV channels, revealing a large dimming effect at and above the limb. The typical 3-part structure observed 1 hour later shows a core shaped similarly to the eruptive filament/prominence. The total measured mass of the escaping CME (1.5x10to16 g from C2 LASCO observations) definitely exceeds the estimated mass of the escaping cool prominence material although assumptions made to analyse the Ha erupting prominence, as well as the corresponding EUV darkening of the filament observed several days before, made this evaluation uncertain by a factor of 2. From the current free extrapolation we discuss the shape of the magnetic neutral surface and a possible scenario leading to an instability, including the small scale dynamics inside and around the filament.
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